Table 1: Properties of isolated static neutron stars of gravitational mass $M=1.35~{M}_\odot$ for the three EOSs used in our computations. $M/R\equiv GM/Rc^2$ is the compaction parameter, R is the areal radius, $M_{\rm B}$ is the baryon mass and $\rho _{\rm c}$ is the central energy density, respectively.
EOS M/R $R~[{\rm km}]$ $M_{\rm B} [M_{\odot}]$ $\rho_{\rm c}~[10^{14}{\rm g/cm^3}]$

GNH3 0.140 14.262 1.45351 6.26

APR 0.176 11.350 1.49110 9.80

BPAL12 0.191 10.447 1.48472 20.22

**Table 1:** Properties of isolated static neutron stars of gravitational mass $M=1.35~{M}_\odot$ for the three EOSs used in our computations. $M/R\equiv GM/Rc^2$ is the compaction parameter, R is the areal radius, $M_{\rm B}$ is the baryon mass and $\rho _{\rm c}$ is the central energy density, respectively.
EOS	M/R	$R~[{\rm km}]$	$M_{\rm B} [M_{\odot}]$	$\rho_{\rm c}~[10^{14}{\rm g/cm^3}]$
GNH3	0.140	14.262	1.45351	6.26
APR	0.176	11.350	1.49110	9.80
BPAL12	0.191	10.447	1.48472	20.22

Source LaTeX | All tables | In the text

	1 Introduction
	2 Description of the equations of state
	3 Numerical method
	4 Numerical results
	5 Concluding remarks
	References